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関連する概念動画

Radiation Pressure: Problem Solving01:09

Radiation Pressure: Problem Solving

686
The radiation pressure applied by an electromagnetic wave on a perfectly absorbing surface equals the energy density of the wave. The wave's momentum also gets transferred to the surface when an electromagnetic wave is entirely absorbed by it. The rate at which momentum is transmitted to an absorbing surface perpendicular to the propagation direction equals the force on the surface.
The average value of the rate of momentum transfer divided by the absorbing area represents the average force...
686
Maxwell-Boltzmann Distribution: Problem Solving01:20

Maxwell-Boltzmann Distribution: Problem Solving

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Individual molecules in a gas move in random directions, but a gas containing numerous molecules has a predictable distribution of molecular speeds, which is known as the Maxwell-Boltzmann distribution, f(v).
This distribution function f(v) is defined by saying that the expected number N (v1,v2) of particles with speeds between v1 and v2 is given by
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Calculation of Electric Flux01:25

Calculation of Electric Flux

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Consider the electric field of an oppositely charged, parallel-plate system and an imaginary box between those plates. Let the bottom face of the box be ABCD, and the top face be FGHK. The electric field between the plates is uniform and points from the positive plate toward the negative plate. The calculation of this field's flux through the box's various faces shows that the net flux through the box is zero. Why does the flux cancel out here?
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Momentum And Radiation Pressure01:20

Momentum And Radiation Pressure

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An object absorbing an electromagnetic wave would experience a force in the direction of propagation of the wave. This force occurs because electromagnetic waves contain and transport momentum. The force accounts for the wave's radiation pressure exerted on the object. Maxwell's prediction was confirmed in 1903 by Nichols and Hull by precisely measuring radiation pressures with a torsion balance. The measuring instrument had mirrors suspended from a fiber kept inside a glass container.
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Potential Due to a Magnetized Object01:24

Potential Due to a Magnetized Object

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Magnetic dipoles in magnetic materials are aligned when placed under an external magnetic field. For paramagnets and ferromagnets, dipole alignment occurs in the direction of the magnetic field. However, the dipoles align opposite to the field in the case of diamagnets. This state of magnetic polarization due to the external field is called magnetization. Magnetization is defined as the dipole moment per unit volume. It plays a similar role to polarization in electrostatics.
The vector...
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Potential Due to a Polarized Object01:29

Potential Due to a Polarized Object

648
A neutral atom consists of a positively charged nucleus surrounded by a negatively charged electron cloud. When placed in an external electric field, the external electric force pulls the electrons and nucleus apart, opposite to the intrinsic attraction between the nucleus and the electrons. The opposing forces balance each other with a slight shift between the center of masses of the nucleus and the electron cloud, resulting in a polarized atom. On the other hand, a few molecules, like water,...
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Updated: Dec 13, 2025

Indoor Experimental Assessment of the Efficiency and Irradiance Spot of the Achromatic Doublet on Glass ADG Fresnel Lens for Concentrating Photovoltaics
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物理 に 基づく 方法 で,差し迫っ て いる 大きな 太陽 フレア を 予測 できる

Kanya Kusano1, Tomoya Iju2, Yumi Bamba3,4

  • 1Institute for Space-Earth Environmental Research, Nagoya University, Nagoya 464-8601, Japan. kusano@nagoya-u.jp.

Science (New York, N.Y.)
|August 1, 2020
PubMed
まとめ
この要約は機械生成です。

新しい物理ベースのモデルである κ-スキームは,重要な磁気動力学的不安定性を特定することによって,大きな太陽フレアを正確に予測します. このモデルは磁気回転フルス密度を使用して,フレア発生,位置,サイズを決定し,宇宙天気予報を改善します.

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Simulating Imaging of Large Scale Radio Arrays on the Lunar Surface
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関連する実験動画

Last Updated: Dec 13, 2025

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Simulating Imaging of Large Scale Radio Arrays on the Lunar Surface
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Scattering And Absorption of Light in Planetary Regoliths
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Scattering And Absorption of Light in Planetary Regoliths

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科学分野:

  • * 太陽物理学
  • * 宇宙天気
  • * プラズマ物理学

背景:

  • * 太陽フレアは地球の宇宙天候に影響を与えるエネルギー的な冠状の出来事です.
  • * 現在の太陽フレア予測は,未知の発生メカニズムによる経験的方法に依存しています.
  • * フレアトリガーの理解は,予測能力を改善するために不可欠です.

研究 の 目的:

  • * 大きな太陽フレアを予測するための物理ベースのモデル, κ-スキームを導入する.
  • * マグネト・ヒドロダイナミック 不安定性と磁気再接続がフレア開始における役割を調査する.
  • * フレアの発生,位置,大きさを決定する重要なパラメータを特定する.

主な方法:

  • * 物理に基づく予測モデルである κ-スキーマの開発.
  • * 2008年から2019年までのX級太陽フレアの分析 (太陽周期24).
  • * 極性逆転線付近の磁気回転フルス密度の試験

主要な成果:

  • * k-スキームは,最も近い大規模な太陽フレアを成功裏に予測します.
  • * 限られた数のフレアは,モデルの予測に例外でした.
  • * 極性逆転線近くの磁気回転フルス密度は重要な予測要因である.

結論:

  • * κ-スキームは,太陽フレアの予測に物理に基づいたアプローチを提供します.
  • * 磁気回転フルースの密度は,太陽フレアの特性を決定する重要な要因です.
  • * この研究は,太陽のフレアメカニズムと予測の理解を進める.